Details

Autor(en) / Beteiligte

• Padilla Gonzalez, E.
• Howell, D. A.
• Terreran, G.
• McCully, C.
• Newsome, M.
• Burke, J.
• Farah, J.
• Pellegrino, C.
• Bostroem, K. A.
• Hosseinzadeh, G.
• Pearson, J.
• Sand, D. J.
• Shrestha, M.
• Smith, N.
• Dong 董, Y. 一泽
• Meza Retamal, N.
• Valenti, S.
• Boos, S.
• Shen, K. J.
• Townsley, D.
• Galbany, L.
• Piscarreta, L.
• Foley, R. J.
• Bustamante-Rosell, M. J.
• Coulter, D. A.
• Chornock, R.
• Davis, K. W.
• Dickinson, C. B.
• Jones, D. O.
• Kutcka, J.
• Le Saux, X. K.
• Rojas-Bravo, C. R.
• Taggart, K.
• Tinyanont, S.
• Yang, G.
• Jha, S. W.
• Margutti, R.

Titel

SN 2022joj: A Potential Double Detonation with a Thin Helium Shell

Ist Teil von

• The Astrophysical journal, 2024-04, Vol.964 (2), p.196

Ort / Verlag

Philadelphia: IOP Publishing

Erscheinungsjahr

2024

Link zum Volltext

Quelle

Free E-Journal (出版社公開部分のみ）

Beschreibungen/Notizen

• Abstract We present photometric and spectroscopic data for SN 2022joj, a nearby peculiar Type Ia supernova (SN Ia) with a fast decline rate (Δ m 15,B = 1.4 mag). SN 2022joj shows exceedingly red colors, with a value of approximately B − V ≈ 1.1 mag during its initial stages, beginning from 11 days before maximum brightness. As it evolves, the flux shifts toward the blue end of the spectrum, approaching B − V ≈ 0 mag around maximum light. Furthermore, at maximum light and beyond, the photometry is consistent with that of typical SNe Ia. This unusual behavior extends to its spectral characteristics, which initially displayed a red spectrum and later evolved to exhibit greater consistency with typical SNe Ia. Spectroscopically, we find strong agreement between SN 2022joj and double detonation models with white dwarf masses of around 1 M ⊙ and a thin He shell between 0.01 and 0.05 M ⊙ . Moreover, the early red colors are explained by line-blanketing absorption from iron peak elements created by the double detonation scenario in similar mass ranges. The nebular spectra in SN 2022joj deviate from expectations for double detonation, as we observe strong [Fe iii ] emission instead of [Ca ii ] lines as anticipated, though this is not as robust a prediction as early red colors and spectra. The fact that as He shells get thinner these SNe start to look more like normal SNe Ia raises the possibility that this is the triggering mechanism for the majority of SNe Ia, though evidence would be missed if the SNe are not observed early enough.